The stellar mass function of quiescent galaxies in 2 < z < 2.5 protoclusters

被引：2

作者：

Edward A.H. ^{[1
,2
]}

Balogh M.L. ^{[1
,2
]}

Bahe Y.M. ^{[3
,4
]}

Cooper M.C. ^{[5
]}

Hatch N.A. ^{[6
]}

Marchioni J. ^{[1
,2
]}

Muzzin A. ^{[4
,7
]}

Noble A. ^{[8
]}

Rudnick G.H. ^{[9
]}

Vulcani B. ^{[10
]}

Wilson G. ^{[11
]}

De Lucia G. ^{[12
]}

Demarco R. ^{[13
]}

Forrest B. ^{[14
]}

Hirschmann M. ^{[15
]}

Castignani G. ^{[16
,17
]}

Cerulo P. ^{[18
]}

Finn R.A. ^{[19
]}

Hewitt G. ^{[1
,2
]}

Jablonka P. ^{[20
,21
]}

Kodama T. ^{[22
]}

Maurogordato S. ^{[23
]}

Nantais J. ^{[24
]}

Xie L. ^{[25
]}

机构：

[1] Department of Physics and Astronomy, University of Waterloo, Waterloo, N2L 3G1, ON

[2] Waterloo Centre for Astrophysics, University of Waterloo, Waterloo, N2L3G1, ON

[3] Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Federale de Lausanne (EPFL), Observatoire de Sauverny, Versoix

[4] Leiden Observatory, Leiden University, P.O. Box 9513, Leiden

[5] Department of Physics and Astronomy, University of California, Irvine, 4129 Frederick Reines Hall, Irvine, 92697, CA

[6] School of Physics and Astronomy, University of Nottingham, Nottingham

[7] Department of Physics and Astronomy, York University, 4700, Keele Street, Toronto, MJ3 1P3, ON

[8] School of Earth and Space Exploration, Arizona State University, Tempe, 85287, AZ

[9] Department of Physics and Astronomy, University of Kansas, Lawrence, 66045, KS

[10] INAF - Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, Padova

[11] Department of Physics, University of California Merced, 5200 Lake Road, Merced, 95343, CA

[12] INAF - Astronomical Observatory of Trieste, via G.B. Tiepolo 11, Trieste

[13] Departamento de Astronomía, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción, Casilla 160-C, Concepción

[14] Department of Physics and Astronomy, University of California Davis, One Shields Avenue, Davis, 95616, CA

[15] Institute for Physics, Laboratory for Galaxy Evolution and Spectral Modelling, Ecole Polytechnique Federale de Lausanne, Observatoire de Sauverny, Chemin Pegasi 51, Versoix

[16] Dipartimento di Fisica e Astronomia 'Augusto Righi, Alma Mater Studiorum Universitá di Bologna, Via Gobetti 93/2, Bologna

[17] INAF - Osservatorio di Astrofisica e Scienza Dello Spazio di Bologna, via Gobetti 93/3, Bologna

[18] Departamento de Ingeniería Informática y Ciencias de la Computaciíon, Facultad de Ingeniería, Universidad de Concepción, Casilla, Concepción

[19] Department of Physics and Astronomy, Siena College, 515 Loudon Rd, Loudonville, 12211, NY

[20] Laboratoire d'Astrophysique, École Polytechnique Federale de Lausanne (EPFL), Sauverny

[21] GEPI, Observatoire de Paris, Universite PSL, CNRS, Place Jules Janssen, Meudon

[22] Astronomical Institute, Tohoku University, 6-3, Aramaki, Aoba, Sendai, Miyagi

[23] Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, Bd de l'Observatoire, Universite Côte d'Azur, CS 34229 Cedex 4, Nice

[24] Instituto de Astrofísica, Departamento de Ciencias Físicas, Universidad Andres Bello, Fernandez Concha 700, Las Condes Región Metropolitana, Santiago

[25] Tianjin Astrophysics Center, Tianjin Normal University, Binshuixidao 393, Tianjin

来源：

Monthly Notices of the Royal Astronomical Society | 2024年 / 527卷 / 03期

基金：

美国国家航空航天局; 美国国家科学基金会; 加拿大自然科学与工程研究理事会;

关键词：

galaxies: clusters: general; galaxies: evolution;

D O I：

10.1093/mnras/stad3751

中图分类号：

学科分类号：

摘要：

We present an analysis of the galaxy stellar mass function (SMF) of 14 known protoclusters between 2.0 < z < 2.5 in the COSMOS field, down to a mass limit of 109.5 M. We use existing photometric redshifts with a statistical background subtraction, and consider star-forming and quiescent galaxies identified from (NUV - r) and (r - J) colours separately. Our fiducial sample includes galaxies within 1 Mpc of the cluster centres. The shape of the protocluster SMF of star-forming galaxies is indistinguishable from that of the general field at this redshift. Quiescent galaxies, however, show a flatter SMF than in the field, with an upturn at low mass, though this is only significant at ∼2σ. There is no strong evidence for a dominant population of quiescent galaxies at any mass, with a fraction <15 per cent at 1σ confidence for galaxies with log M∗/M < 10.5. We compare our results with a sample of galaxy groups at 1 < z < 1.5, and demonstrate that a significant amount of environmental quenching must take place between these epochs, increasing the relative abundance of high-mass () quiescent galaxies by a factor 2. However, we find that at lower masses (), no additional environmental quenching is required. © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

引用

页码：8598 / 8617

页数：19

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